562 research outputs found
Elimination by necrosis, not apoptosis, of mutant embryonic mouse muscle fibers deficient in excitation-contraction coupling.
No full textKuschel T, Heimann P, Heising S, Jockusch H. Elimination by necrosis, not apoptosis, of mutant embryonic mouse muscle fibers deficient in excitation-contraction coupling. Eur J Cell Biol. 1996;69(42):109-114
Timing and location of spawning by bull trout and kokanee in the Odell Lake Watershed and Heising Spring of the Metolius River Watershed, 2003-04
No full textTitle from PDF title page (viewed on November 9, 2018)."Sport Fish Restoration Project F-136R-16."This archived document is maintained by the State Library of Oregon as part of the Oregon Documents Depository Program. It is for informational purposes and may not be suitable for legal purposes.Includes bibliographical references (pages 13-14).Mode of access: Internet from the Oregon Government Publications Collection.Text in English
Mutual interference of myotonia and muscular dystrophy in the mouse: A study on ADR-MDX double mutants
No full textHeimann P, Augustin M, Wieneke S, Heising S, Jockusch H. Mutual interference of myotonia and muscular dystrophy in the mouse: A study on ADR-MDX double mutants. Neuromuscular disorders. 1998;8(8):551-560.For Duchenne muscular dystrophy (DMD, dystrophin deficiency) and Thomsen/Becker myotonia (muscular chloride channel deficiency) genetically homologous mouse models are available, the dystrophin-deficient MDX mouse and the myotonic ADR mouse. Whereas the latter shows more severe symptoms than human myotonia patients, the MDX mouse, in contrast to DMD patients, is only mildly affected. We have introduced, by appropriate breeding, the defect leading to myotonia (Clc1 null mutation, ndr allele) into MDX mice, thus creating ADR-MDX double mutants. The expectation was that, due to mechanical stress during myotonic cramps, the ADR status should symptomatically aggravate the muscle fibre necrosis caused by the dystrophin deficiency. The overall symptoms of the double mutants were dominated by myotonia. Weight reduction and premature death rate were higher in ADR-MDX than in ADR mice. Sarcolemmal ruptures as indicated by influx into muscle fibres of serum globulins and injected Evans blue were found with great inter-individual variation in MDX and in ADR-MDX muscles. Affected fibres were found mainly in large groups in MDX but single or in small clusters in ADR-MDX leg muscles. The symptoms of myotonia (aftercontractions, shift towards oxidative fibres) were less pronounced in ADR-MDX than in ADR muscles. Conversely, numbers of damaged fibres as well as the percentage of central nuclei (an indicator of fibre regeneration) were significantly lower in ADR-MDX than in MDX skeletal muscles. Thus it appears that, at the level of the muscle fibre, myotonia and muscular dystrophy attenuate each other. (C) 1998 Elsevier Science B.V. All rights reserved
Evidence for Low-level Dynamical Excitation in Near-resonant Exoplanet Systems
No full textFull list of the authors: Rice, Malena; Wang, Xian-Yu; Wang, Songhu; Shporer, Avi; Barkaoui, Khalid; Brahm, Rafael; Collins, Karen A.; Jordán, Andrés; Lowson, Nataliea; Butler, R. Paul; Crane, Jeffrey D.; Shectman, Stephen; Teske, Johanna K.; Osip, David; Collins, Kevin I.; Murgas, Felipe; Boyle, Gavin; Pozuelos, Francisco J.; Timmermans, Mathilde; Jehin, Emmanuel; Gillon, MichaëlThe geometries of near-resonant planetary systems offer a relatively pristine window into the initial conditions of exoplanet systems. Given that near-resonant systems have likely experienced minimal dynamical disruptions, the spin-orbit orientations of these systems inform the typical outcomes of quiescent planet formation, as well as the primordial stellar obliquity distribution. However, few measurements have been made to constrain the spin-orbit orientations of near-resonant systems. We present a Rossiter-McLaughlin measurement of the near-resonant warm Jupiter TOI-2202 b, obtained using the Carnegie Planet Finder Spectrograph on the 6.5 m Magellan Clay Telescope. This is the eighth result from the Stellar Obliquities in Long-period Exoplanet Systems survey. We derive a sky-projected 2D spin-orbit angle λ = 26 − 15 + 12 ° and a 3D spin-orbit angle ψ = 31 − 11 + 13 ° , finding that TOI-2202 b—the most massive near-resonant exoplanet with a 3D spin-orbit constraint to date—likely deviates from exact alignment with the host star’s equator. Incorporating the full census of spin-orbit measurements for near-resonant systems, we demonstrate that the current set of near-resonant systems with period ratios P /P ≲ 4 is generally consistent with a quiescent formation pathway, with some room for low-level (≲20°) protoplanetary disk misalignments or post-disk-dispersal spin-orbit excitation. Our result constitutes the first population-wide analysis of spin-orbit geometries for near-resonant planetary systems. © 2023. The Author(s). Published by the American Astronomical Society.We thank the anonymous referee for their valuable feedback on this manuscript. We thank Chelsea Huang for the support in organizing observations for this work. M.R. and S.W. thank the Heising-Simons Foundation for their generous support. M.R. acknowledges support from Heising-Simons Foundation Grant #2023-4478, as well as the 51 Pegasi b Fellowship Program. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. A.J. acknowledges support from ANID-Millennium Science Initiative-ICN12_009 and FONDECYT project 1210718. R.B. acknowledges support from FONDECYT project 11200751 and additional support from ANID-Millennium Science Initiative-ICN12_009
Testing General Relativity with Stellar Orbits around the Supermassive Black Hole in Our Galactic Center
No full textWe demonstrate that short-period stars orbiting around the supermassive black hole in our Galactic center can successfully be used to probe the gravitational theory in a strong regime. We use 19 years of observations of the two best measured short-period stars orbiting our Galactic center to constrain a hypothetical fifth force that arises in various scenarios motivated by the development of a unification theory or in some models of dark matter and dark energy. No deviation from general relativity is reported and the fifth force strength is restricted to an upper 95% confidence limit of |α|<0.016 at a length scale of λ=150 astronomical units. We also derive a 95% confidence upper limit on a linear drift of the argument of periastron of the short-period star S0-2 of |ω S0-2|<1.6×10-3 rad/yr, which can be used to constrain various gravitational and astrophysical theories. This analysis provides the first fully self-consistent test of the gravitational theory using orbital dynamic in a strong gravitational regime, that of a supermassive black hole. A sensitivity analysis for future measurements is also presented.A. H. thanks W. Folkner and P. Wolf for the interesting discussions. Support for this work was provided by NSF Grant No. AST-1412615, the Heising-Simon Foundation, the Levine-Leichtman Family Foundation, the Galactic Center Board of Advisors, and Janet Marott for her support of the research on S0-38 through the Galactic Center Stellar Patron Program
Circumstellar Medium Constraints on the Environment of Two Nearby Type Ia Supernovae: SN 2017cbv and SN 2020nlb
No full textWe present deep Chandra X-ray observations of two nearby Type Ia supernovae, SN 2017cbv and SN 2020nlb, which reveal no X-ray emission down to a luminosity LX ≲ 5.3 × 1037 and ≲ 5.4 × 1037 erg s-1 (0.3-10 keV), respectively, at ∼16-18 days after the explosion. With these limits, we constrain the pre-explosion mass-loss rate of the progenitor system to be Ṁ < 7.2 × 10-9 and < 9.7 × 10-9 M⊙ yr-1 for each (at a wind velocity v w = 100 km s-1 and a radius of R ≈ 1016 cm), assuming any X-ray emission would originate from inverse Compton emission from optical photons upscattered by the supernova shock. If the supernova environment was a constant-density medium, we would find a number density limit of nCSM < 36 and < 65 cm-3, respectively. These X-ray limits rule out all plausible symbiotic progenitor systems, as well as large swathes of parameter space associated with the single degenerate scenario, such as mass loss at the outer Lagrange point and accretion winds. We also present late-time optical spectroscopy of SN 2020nlb, and set strong limits on any swept up hydrogen (LHα < 2.7 × 1037 erg s-1) and helium (LHe,λ6678 < 2.7 × 1037 erg s-1) from a nondegenerate companion, corresponding to MH ≲ 0.7-2 × 10-3 M⊙ and MHe ≲ 4 × 10-3 M⊙. Radio observations of SN 2020nlb at 14.6 days after explosion also yield a non-detection, ruling out most plausible symbiotic progenitor systems. While we have doubled the sample of normal Type Ia supernovae with deep X-ray limits, more observations are needed to sample the full range of luminosities and subtypes of these explosions, and set statistical constraints on their circumbinary environments.Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number DDO-21119X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. This work makes use of observations from the Las Cumbres Observatory network. The LCO team is supported by NSF grants AST-1911225 and AST-1911151 and NASA Swift grant 80NSSC19K1639. Research by S.V. is supported by NSF grants AST-1813176 and AST-2008108. Time domain research by D.J.S. is also supported by NSF grants AST-1821987, 1813466, 1908972, and 2108032, and by the Heising-Simons Foundation under grant No. 2020-1864. S.K.S. and L.C. are supported by NSF grant AST-1907790 and the Packard Foundation. L.G. acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under the 2019 Ramón y Cajal program RYC2019-027683 and from the Spanish MICIU project PID2020-115253GA-I00. L.W. is sponsored (in part) by the Chinese Academy of Sciences (CAS) through a grant to the CAS South America Center for Astronomy (CASSACA) in Santiago, Chile
Toward pillared layered metal sulfides. Intercalation of the chalcogenide clusters Co(6)Q(8)(PR(3))(6) (Q=S, Se, and Te and R=alkyl) into MoS2
No full textA new family of materials based on layered transition metal dichalcogenides of the type [M'(x)Q(y)L(z)](n)[MoS2] (Q = S, Se, Te) was prepared as a first step toward pillared layered sulfides. The new intercalated phases form from the addition of Co(6)Q(8)(PR(3))(6) solutions to exfoliated suspensions MoS2.Source type: Electronic(1
Canton, Ohio
No full textSTREETS: Camden Ave. S. W. [1300-1319]; Fourteenth St. S. W. [1401-1625]; Gayle Place S. W. [1400-1625]; Heising Court S. W. [1300-1385]; Henry Ave. S. W. [1300-1402]; Margaret Ave. S. W. [1301-1399]; Navarre Road S. W. [1300-1626]; Pearl Place S. W. [1400-1625]; Race Court S. W. [1300-1399]; Scoville Ave. S. W. [1300-1398]; Stark Ave. S. W. [1300-1399]; SPECIALS: All Saints Polish Catholic Church; Trinity Evangelical United Brethren Churc
Drought Effects on Tectona grandis Water Regulation Are Mediated by Thinning, but the Effects of Thinning Are Temporary
No full text10 páginas.- 5 figuras.- referencias.- The Supplementary Material for this article can be found online at: https://www.frontiersin.org/articles/10.3389/ffgc.2019.00082/full#supplementary-materialResults from tropical planted forests have demonstrated that tree plantations can have variable growth and water use patterns in response to drought. Yet research on how specific species will perform during a drought and whether this response can be mediated through forest management is still poorly understood. We took advantage of the 2015¿2016 El Niño drought in central Panama to test the effects of thinning on sap flux density, transpiration, and growth of planted Tectona grandis (teak), a non-native species introduced to Panama for timber production. Despite a reduction in growth of teak during drought for control and thinned sites, tree sap flux density of thinned sights significantly increased after thinning, but the effect was temporary. Sap flux density (Js) for teak is strongly driven by changes in vapor pressure deficit (VPD), temperature, and radiation; however, Js declines as temperature rises above 28°C and VPD is above 0.5, suggesting a temperature threshold that could be problematic as droughts and temperatures increase in unison in the future. At the stand-level, all sites reduced transpiration during the drought. Although diameter growth and transpiration declined during drought, the leaf area index after the drought ended returned to pre-drought levels.KS was supported by grants and fellowships from the Smart Reforestation® program of the Smithsonian Tropical Research Institute, Mr. Stanley Motta, the Silicon Valley Foundation, the Heising-Simons Foundation, and the University of New Hampshire. CB was supported by grants and fellowships from the Smithsonian Tropical Research Institute and the University of New Hampshire International Research Opportunities Program
The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. III. Aperture Masking Interferometric Observations of the Star HIP 65426 at 3.8μm
No full textRay, Shrishmoy et al.-- Full list of authors: Ray, Shrishmoy; Sallum, Steph; Hinkley, Sasha; Sivaramkrishnan, Anand; Cooper, Rachel; Kammerer, Jens; Greebaum, Alexandra Z.; Thatte, Deeparshi; Stolker, Tomas; Lazzoni, Cecilia; Tokovinin, Andrei; de Furio, Matthew; Factor, Samuel; Meyer, Michael; Stone, Jordan M.; Carter, Aarynn; Biller, Beth; Skemer, Andrew; Suárez, Genaro; Leisenring, Jarron M.; Perrin, Marshall D.; Kraus, Adam L.; Absil, Olivier; Balmer, William O.; Boccaletti, Anthony; Bonavita, Mariangela; Bonnefoy, Mickael; Booth, Mark; Bowler, Brendan P.; Briesemeister, Zackery W.; Bryan, Marta L.; Calissendorff, Per; Cantalloube, Faustine; Chauvin, Gael; Chen, Christine H.; Choquet, Elodie; Christiaens, Valentin; Cugno, Gabriele; Currie, Thayne; Danielski, Camilla; Dupuy, Trent J.; Faherty, Jacqueline K.; Fitzgerald, Michael P.; Fortney, Jonathan J.; Franson, Kyle; Girard, Julien H.; Grady, Carol A.; Gonzales, Eileen C.; Henning, Thomas; Hines, Dean C.; Hoch, Kielan K. W.; Hood, Callie E.; Howe, Alex R.; Janson, Markus; Kalas, Paul; Kennedy, Grant M.; Kenworthy, Matthew A.; Kervella, Pierre; Kuzuhara, Masayuki; Lagrange, Anne-Marie; Lagage, Pierre-Olivier; Lawson, Kellen; Lew, Ben W. P.; Liu, Michael C.; Liu, Pengyu; Llop-Sayson, Jorge; Lloyd, James P.; Macintosh, Bruce; Marino, Sebastian; Marley, Mark S.; Marois, Christian; Martinez, Raquel A.; Matthews, Brenda C.; Matthews, Elisabeth C.; Mawet, Dimitri; Mazoyer, Johan; McElwain, Michael W.; Metchev, Stanimir; Meyer, Michael R.; Miles, Brittany E.; Millar-Blanchaer, Maxwell A.; Molliere, Paul; Moran, Sarah E.; Morley, Caroline V.; Mukherjee, Sagnick; Palma-Bifani, Paulina; Pantin, Eric; Patapis, Polychronis; Petrus, Simon; Pueyo, Laurent; Quanz, Sascha P.; Quirrenbach, Andreas; Rebollido, Isabel; Adams Redai, Jea; Ren, Bin B.; Rickman, Emily; Samland, Matthias; Schlieder, Joshua E.; Schneider, Glenn; Stapelfeldt, Karl R.; Tamura, Motohide; Tan, Xianyu; Uyama, Taichi; Vigan, Arthur; Vasist, Malavika; Vos, Johanna M.; Wagner, Kevin; Wang, Jason J.; Ward-Duong, Kimberly; Whiteford, Niall; Wolff, Schuyler G.; Worthen, Kadin; Wyatt, Mark C.; Ygouf, Marie; Zhang, Xi; Zhang, Keming; Zhang, Zhoujian; Zhou, Yifan; Zurlo, Alice; Sargent, B. A.; Theissen, Christopher A.; Manjavacas, Elena; Lueber, Anna; Kitzmann, Daniel; Sutlieff, Ben J.; Betti, Sarah K.We present aperture masking interferometry (AMI) observations of the star HIP 65426 at 3.8 μm, as part of the JWST Direct Imaging Early Release Science program, obtained using the Near Infrared Imager and Slitless Spectrograph instrument. This mode provides access to very small inner working angles (even separations slightly below the Michelson limit of 0.5λ/D for an interferometer), which are inaccessible with the classical inner working angles of the JWST coronagraphs. When combined with JWST's unprecedented infrared sensitivity, this mode has the potential to probe a new portion of parameter space across a wide array of astronomical observations. Using this mode, we are able to achieve a 5σ contrast of ΔmF380M ∼ 7.62 ± 0.13 mag relative to the host star at separations ≳0
07, and the contrast deteriorates steeply at separations ≲0
07. However, we detect no additional companions interior to the known companion HIP 65426b (at separation ∼0
82 or
). Our observations thus rule out companions more massive than 10–12 MJup at separations ∼10–20 au from HIP 65426, a region out of reach of ground- or space-based coronagraphic imaging. These observations confirm that the AMI mode on JWST is sensitive to planetary mass companions at close-in separations (≳0
07), even for thousands of more distant stars at ∼100 pc, in addition to the stars in the nearby young moving groups and associations, as stated in previous works. This result will allow the planning and successful execution of future observations to probe the inner regions of nearby stellar systems, opening an essentially unexplored parameter space. © 2025. The Author(s).This work is based on observations made with the NASA/
ESA/CSA JWST and obtained from the Mikulski Archive for
Space Telescopes at the Space Telescope Science Institute. The
specific observations analyzed can be accessed via 10.17909/
8by2-x206. We are truly grateful for the countless hours that
thousands of people have devoted to the design, construction,
and commissioning of JWST. We thank the anonymous referee
for comments that have been crucial toward the improvement
of this Letter. This project was supported by a grant from
STScI (JWST-ERS-01386) under NASA contract NAS5-
03127. S.R. was supported by the Global Excellence Award
at the University of Exeter. This work is based in part on
observations obtained at the Southern Astrophysical Research
(SOAR) telescope, which is a joint project of the Ministério da
Ciência, Tecnologia e Inovações (MCTI/LNA) of Brasil, the
US National Science Foundation’s NOIRLab, the University of
North Carolina at Chapel Hill (UNC), and Michigan State
University (MSU). This work has also made use of the
SPHERE Data Centre, jointly operated by OSUG/IPAG
(Grenoble), PYTHEAS/LAM/CeSAM (Marseille), OCA/
Lagrange (Nice), Observatoire de Paris/LESIA (Paris), and
Observatoire de Lyon/CRAL, as well as being supported by a
grant from Labex OSUG@2020 (Investissements d’avenir—
ANR10 LABX56). This work has benefited from the 2022
Exoplanet Summer Program in the Other Worlds Laboratory
(OWL) at the University of California, Santa Cruz, a program
funded by the Heising–Simons Foundation.Peer reviewe
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